What are protostellar outflows are

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Protostellar envelope : - Cold (10K), outer envelope : molecular depletion, superdeuteration Size : 10 4 AU Warm (100K), inner envelope : hot corino : grain mantle sublimation, rich molecular complexity Size : 100 AU HH399 in M20 (Lefloch et al. 2002) Mass-loss phenomena : Outflows High-velocity, highly-collimated ionic/atomic jet Molecular Jet – several 100 km/s Knotty structure Low-velocity (10km/s), extended, molecular rich, outflow cavity (10K). Wide-angle wind ? Shocks in the envelope and the ambient cloud Van Dishoeck et al. (2010) COSPAR 2012 - Outflows - B. Lefloch
What are protostellar outflows are ? are they observed at all stages of protostellar evolution ? what are the physical conditions in the outflowing gas : T ? n ? size ? Mass ? (and how do they vary with protostellar evolution and the protostar) ? What is the origin of molecules in protostellar outflows and jets ? How the gas is accelerated up to several 100 km/s ? What is the relation (if any) between the different outflow phenomena ? What is the impact of outflows on the parental core (cloud) and are they dynamically important at all ? What is the role of outflows in the molecular gas complexity ? Positive/Negative impact ? COSPAR 2012 - Outflows - B. Lefloch
Page 1 and 2: Bertrand Lefloch IPAG, Grenoble, Fr
Page 3: Herbig 1950, 1951; Haro 1952, 1953
Page 7 and 8: Outflows • Precess - increases in
Page 9 and 10: IRAS 20126+4104 Cesaroni et al. (19
Page 11 and 12: Mass-velocity relation exhibits bro
Page 13 and 14: Evolution: opening angle widens wit
Page 15 and 16: A few contributions: Turbulent jet:
Page 17 and 18: HH212: consistent with jet-driving
Page 19 and 20: Ciardi & Hennebelle (2010) COSPAR 2
Page 21 and 22: Shocks are dynamically important :
Page 23 and 24: Outflows interact with the parental
Page 25 and 26: H 2 C-shock J-shock MIR NIR SiO SED
Page 27 and 28: 2.12µm Optical size ~ 2’’ (a f
Page 29 and 30: dN T -a B1 position Nisini et al.
Page 31 and 32: Flower & Pineau des Forets (2010) H
Page 33 and 34: Chemically active outflows L1157 (B
Page 35 and 36: Bachiller et al. (2001) Gueth et al
Page 37 and 38: Rodriguez-Fernandez et al. in prep
Page 39 and 40: PACS HIFI : 490 - 1900 GHz. 27 hrs.
Page 41 and 42: Species detected CO, 13 CO, C 18 O
Page 43 and 44: PACS Spectrum : CO (J up = 14 - 22)
Page 45 and 46: CO : IRAM, CSO, HIFI HIFI Lefloch e
Page 47 and 48: C-type CO Direct evidence for 2 sho
Page 49 and 50: ISO detected strong H 2 O emission
Page 51 and 52: Extended H 2 O emission CSO 325 GHz
Page 53 and 54: B R SiO B R SiO SiO 2-1 Lefloch et
Page 55 and 56:
COSPAR 2012 - Outflows - B. Lefloch
Page 57 and 58:
Page 59 and 60:
DG Tau red blue Testi et al. 2002 J
Page 61 and 62:
Origin of molecules in jets ? Sever
Page 63 and 64:
Page 65:
A total of 11 emission lines (E up
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What are protostellar outflows are

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